Table 5: Parameters for the spectral energy distribution for the first and second week of the campaign. p₁ and p₂ are the pre and post break spectral index for the electron population, $\gamma ^*$ is the break energy Lorentz factor, $\gamma _{\rm min}$ is the cut-off energy of the electron population, B the tangled magnetic field, r the radius of the spherical blob in the comoving frame, $\delta$ the Doppler factor, $n_{\rm e}$ the electron density.
Week p₁ p₂ $\gamma ^*$ $\gamma _{\rm min}$ B r $\delta$ Disk Luminosity $n_{\rm e}$

(Gauss) (10¹⁶ cm) ( $10^{45} ~ \rm erg~ cm^{-2}~ s^{-1}$ ) (e $^-/\rm cm^3$ )

First 2 5 200 3 12 2 9 6 150

Second 2 4.7 300 3 10 2 9 6 $\ 70$

**Table 5:** Parameters for the spectral energy distribution for the first and second week of the campaign. p₁ and p₂ are the pre and post break spectral index for the electron population, $\gamma ^*$ is the break energy Lorentz factor, $\gamma _{\rm min}$ is the cut-off energy of the electron population, B the tangled magnetic field, r the radius of the spherical blob in the comoving frame, $\delta$ the Doppler factor, $n_{\rm e}$ the electron density.
Week	p₁	p₂	$\gamma ^*$	$\gamma _{\rm min}$	B	r	$\delta$	Disk Luminosity	$n_{\rm e}$
					(Gauss)	(10¹⁶ cm)		( $10^{45} ~ \rm erg~ cm^{-2}~ s^{-1}$ )	(e $^-/\rm cm^3$ )
First	2	5	200	3	12	2	9	6	150
Second	2	4.7	300	3	10	2	9	6	$\ 70$

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